The data are reduced with the standard PCWI pipeline
[1]}. The flux calibration was performed
using the standard star BD\(+\) 28D4211, observed on the same
night, and the final datacube is combined by weighting individual
exposures according to their inverse variance. In addition, the
wavelengths are converted into their values in vacuum. The final
cube has a pixel size of \(\sim 1.5\)  arcsec in the spatial direction,
and 0.55 Å in the wavelength direction. In addition, the spatial
resolution of PCWI cube is seeing limited along the slices in the
short direction, which at the time of observations was \( 1.4\) 
arcsec, and slit limited (\(\sim \)  2.5 arcsec) in the long direction.
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